o - Salem State University
... Visible, UV, X-rays, gamma rays Visible, microwave, radio, infrared Infrared, visible, radio, X-rays ...
... Visible, UV, X-rays, gamma rays Visible, microwave, radio, infrared Infrared, visible, radio, X-rays ...
Earth Science 11 Chapter 28 Answers: 28.1 1. All are forms of
... active galaxy emits far more energy than the sum of energy emitted by its component stars. Active galaxies emit large amounts of energy and/or are highly variable and change in brightness over a short period. 4. From top: Observable universe, Virgo Cluster; from left Comets, Planets, Sun, Asteroids, ...
... active galaxy emits far more energy than the sum of energy emitted by its component stars. Active galaxies emit large amounts of energy and/or are highly variable and change in brightness over a short period. 4. From top: Observable universe, Virgo Cluster; from left Comets, Planets, Sun, Asteroids, ...
11.3 Measuring Distances in Space
... The distance to a far away object can be determined by measuring two angles and the distance between those two angles. A line (called a baseline) is laid out and angle measurements are taken at the baseline endpoints to the distant object. Geometry and Trigonometry are then used to determine the per ...
... The distance to a far away object can be determined by measuring two angles and the distance between those two angles. A line (called a baseline) is laid out and angle measurements are taken at the baseline endpoints to the distant object. Geometry and Trigonometry are then used to determine the per ...
STARS- hot glowing sphere of gas that produces energy by
... A) Actual brightness- brightness right next to a star B) Apparent brightness—brightness as seen from earth 3] Formation of stars A) Nebula (cloud of dust and gas) collapses under its own gravity B) Friction in core causes temperature to reach 10,000,000 c C) fusion begins and a star is born 4] How s ...
... A) Actual brightness- brightness right next to a star B) Apparent brightness—brightness as seen from earth 3] Formation of stars A) Nebula (cloud of dust and gas) collapses under its own gravity B) Friction in core causes temperature to reach 10,000,000 c C) fusion begins and a star is born 4] How s ...
Gravitational mass
... •It is interesting that Einstein had included a fudge factor in the General Theory of Relativity called the “Cosmological Constant” that explained the stability of the universe. •When it was discovered that the universe is expanding then the Cosmological Constant was not necessary so Einstein consid ...
... •It is interesting that Einstein had included a fudge factor in the General Theory of Relativity called the “Cosmological Constant” that explained the stability of the universe. •When it was discovered that the universe is expanding then the Cosmological Constant was not necessary so Einstein consid ...
Celestial Bodies (Mike Stroppa) - Powerpoint
... • The star may turn into a neutron star, or a black hole ...
... • The star may turn into a neutron star, or a black hole ...
The Earth in Space
... motions of the earth, and other celestial bodies. 1. Year - is the time it takes for the earth to make one complete orbit around the Sun. 2. Month - is the time it takes for the Moon to go through one full period of phases. ...
... motions of the earth, and other celestial bodies. 1. Year - is the time it takes for the earth to make one complete orbit around the Sun. 2. Month - is the time it takes for the Moon to go through one full period of phases. ...
chapter-30-pp
... slightly toward blue. This is called a “blue shift”. This is caused by shorter light waves as it moves toward Earth. ...
... slightly toward blue. This is called a “blue shift”. This is caused by shorter light waves as it moves toward Earth. ...
2nd Semester Exam Study Guide
... -light emitted shifts toward the red end of the spectrum; shows that the star is moving away from Earth - light shifted toward the blue end of the spectrum; shows that the star is moving toward Earth 6. According to the Big Bang Theory, the universe is expanding and galaxies are moving away from the ...
... -light emitted shifts toward the red end of the spectrum; shows that the star is moving away from Earth - light shifted toward the blue end of the spectrum; shows that the star is moving toward Earth 6. According to the Big Bang Theory, the universe is expanding and galaxies are moving away from the ...
Astronomy Problems – Color Index Nov. 2011
... Astronomy Problems – Color Index Nov. 2011 Colors of Stars Astronomers measure the brightness of stars at three colors of light: The "U" band at 360 nm The "B" band at 440 nm The "V" band at 540 nm The "color index" of a star is defined as the magnitude in the B filter, minus the magnitude in ...
... Astronomy Problems – Color Index Nov. 2011 Colors of Stars Astronomers measure the brightness of stars at three colors of light: The "U" band at 360 nm The "B" band at 440 nm The "V" band at 540 nm The "color index" of a star is defined as the magnitude in the B filter, minus the magnitude in ...
A Dart Board for the Bored An eye opening offer from the editors of
... the Milky Way runs slightly through Cepheus, it contains no Messier objects or other interesting deep sky objects. A star cluster and four nebulas appear in the constellation, but they are faint, however, it does contain a recent visitor to our solar system, Comet Abe. As shown on the map, Comet Abe ...
... the Milky Way runs slightly through Cepheus, it contains no Messier objects or other interesting deep sky objects. A star cluster and four nebulas appear in the constellation, but they are faint, however, it does contain a recent visitor to our solar system, Comet Abe. As shown on the map, Comet Abe ...
New Worlds - Universiteit Leiden
... and fly off at Warp 9 to a distant dust cloud and then raise the temperature or add a few chemical compounds and see what effect this has. All our knowledge is obtained indirectly from the radiation which the objects themselves emit. According to the laws of quantum mechanics, each atom or molecule ...
... and fly off at Warp 9 to a distant dust cloud and then raise the temperature or add a few chemical compounds and see what effect this has. All our knowledge is obtained indirectly from the radiation which the objects themselves emit. According to the laws of quantum mechanics, each atom or molecule ...
Observational astronomy
Observational astronomy is a division of the astronomical science that is concerned with recording data, in contrast with theoretical astrophysics, which is mainly concerned with finding out the measurable implications of physical models. It is the practice of observing celestial objects by using telescopes and other astronomical apparatus.As a science, the study of astronomy is somewhat hindered in that direct experiments with the properties of the distant universe are not possible. However, this is partly compensated by the fact that astronomers have a vast number of visible examples of stellar phenomena that can be examined. This allows for observational data to be plotted on graphs, and general trends recorded. Nearby examples of specific phenomena, such as variable stars, can then be used to infer the behavior of more distant representatives. Those distant yardsticks can then be employed to measure other phenomena in that neighborhood, including the distance to a galaxy.Galileo Galilei turned a telescope to the heavens and recorded what he saw. Since that time, observational astronomy has made steady advances with each improvement in telescope technology.A traditional division of observational astronomy is given by the region of the electromagnetic spectrum observed: Optical astronomy is the part of astronomy that uses optical components (mirrors, lenses and solid-state detectors) to observe light from near infrared to near ultraviolet wavelengths. Visible-light astronomy (using wavelengths that can be detected with the eyes, about 400 - 700 nm) falls in the middle of this range. Infrared astronomy deals with the detection and analysis of infrared radiation (this typically refers to wavelengths longer than the detection limit of silicon solid-state detectors, about 1 μm wavelength). The most common tool is the reflecting telescope but with a detector sensitive to infrared wavelengths. Space telescopes are used at certain wavelengths where the atmosphere is opaque, or to eliminate noise (thermal radiation from the atmosphere). Radio astronomy detects radiation of millimetre to dekametre wavelength. The receivers are similar to those used in radio broadcast transmission but much more sensitive. See also Radio telescopes. High-energy astronomy includes X-ray astronomy, gamma-ray astronomy, and extreme UV astronomy, as well as studies of neutrinos and cosmic rays.Optical and radio astronomy can be performed with ground-based observatories, because the atmosphere is relatively transparent at the wavelengths being detected. Observatories are usually located at high altitudes so as to minimise the absorption and distortion caused by the Earth's atmosphere. Some wavelengths of infrared light are heavily absorbed by water vapor, so many infrared observatories are located in dry places at high altitude, or in space.The atmosphere is opaque at the wavelengths used by X-ray astronomy, gamma-ray astronomy, UV astronomy and (except for a few wavelength ""windows"") far infrared astronomy, so observations must be carried out mostly from balloons or space observatories. Powerful gamma rays can, however be detected by the large air showers they produce, and the study of cosmic rays is a rapidly expanding branch of astronomy.For much of the history of observational astronomy, almost all observation was performed in the visual spectrum with optical telescopes. While the Earth's atmosphere is relatively transparent in this portion of the electromagnetic spectrum, most telescope work is still dependent on seeing conditions and air transparency, and is generally restricted to the night time. The seeing conditions depend on the turbulence and thermal variations in the air. Locations that are frequently cloudy or suffer from atmospheric turbulence limit the resolution of observations. Likewise the presence of the full Moon can brighten up the sky with scattered light, hindering observation of faint objects.For observation purposes, the optimal location for an optical telescope is undoubtedly in outer space. There the telescope can make observations without being affected by the atmosphere. However, at present it remains costly to lift telescopes into orbit. Thus the next best locations are certain mountain peaks that have a high number of cloudless days and generally possess good atmospheric conditions (with good seeing conditions). The peaks of the islands of Mauna Kea, Hawaii and La Palma possess these properties, as to a lesser extent do inland sites such as Llano de Chajnantor, Paranal, Cerro Tololo and La Silla in Chile. These observatory locations have attracted an assemblage of powerful telescopes, totalling many billion US dollars of investment.The darkness of the night sky is an important factor in optical astronomy. With the size of cities and human populated areas ever expanding, the amount of artificial light at night has also increased. These artificial lights produce a diffuse background illumination that makes observation of faint astronomical features very difficult without special filters. In a few locations such as the state of Arizona and in the United Kingdom, this has led to campaigns for the reduction of light pollution. The use of hoods around street lights not only improves the amount of light directed toward the ground, but also helps reduce the light directed toward the sky.Atmospheric effects (astronomical seeing) can severely hinder the resolution of a telescope. Without some means of correcting for the blurring effect of the shifting atmosphere, telescopes larger than about 15–20 cm in aperture can not achieve their theoretical resolution at visible wavelengths. As a result, the primary benefit of using very large telescopes has been the improved light-gathering capability, allowing very faint magnitudes to be observed. However the resolution handicap has begun to be overcome by adaptive optics, speckle imaging and interferometric imaging, as well as the use of space telescopes.Astronomers have a number of observational tools that they can use to make measurements of the heavens. For objects that are relatively close to the Sun and Earth, direct and very precise position measurements can be made against a more distant (and thereby nearly stationary) background. Early observations of this nature were used to develop very precise orbital models of the various planets, and to determine their respective masses and gravitational perturbations. Such measurements led to the discovery of the planets Uranus, Neptune, and (indirectly) Pluto. They also resulted in an erroneous assumption of a fictional planet Vulcan within the orbit of Mercury (but the explanation of the precession of Mercury's orbit by Einstein is considered one of the triumphs of his general relativity theory).